Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period
Autor(a) principal: | |
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Data de Publicação: | 1990 |
Outros Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , |
Tipo de documento: | Artigo |
Idioma: | eng |
Título da fonte: | Repositório Institucional da UFRGS |
Texto Completo: | http://hdl.handle.net/10183/108715 |
Resumo: | Using an extensive set of high-speed photometric observations obtained with the Whole Earth Telescope network, we show that the complex light curve of the ZZ Ceti (DAV) star G29-38 is dominated by a single, constant amplitude period of 615 s during the time span of our observations. The pulse arrival times for this period exhibit a systematic variation in phase readily explained by light-travel time effects produced by reflex orbital motion about an unseen companion. Our best-fit model to the observations indicates a highly eccen tric orbit, a period of 109 ± 13 days and a minimum mass of 0.5 Mʘ for the companion. Radial velocity variations predicted by this model are not observed, however, nor are these phase variations seen in another independent pulsation, so the origin of the phase variation remains a mystery. Any model involving intrinsic pulsation mechanisms must explain the large (~200 s) phase change with no corresponding change in pulsation amplitude, and it shape, which mimics quite exactly the effects of binary orbital motion. |
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Winget, Donald EarlNather, R. EdwardClemens, J. ChristopherProvencal, Judith L.Kleinman, Scot JamesBradley, Paul A.Wood, Matthew A.Claver, C.F.Robinson, E.L.Grauer, Albert D.Hine, B.P.Fontaine, GillesAchilleos, NicholasMarar, T.M. KrishnanSeetha, S.Ashoka, B.N.O'Donoghue, DarraghWarner, B.Kurtz, Donald W.Martinez, PeterVauclair, GérardChevreton, MichelAugusteijn, T.Paradijs, J. vanHansen, Carl J.Liebert, JamesKanaan Neto, Antonio NemerKepler, Souza Oliveira2014-12-31T02:10:48Z19900004-637Xhttp://hdl.handle.net/10183/108715000015354Using an extensive set of high-speed photometric observations obtained with the Whole Earth Telescope network, we show that the complex light curve of the ZZ Ceti (DAV) star G29-38 is dominated by a single, constant amplitude period of 615 s during the time span of our observations. The pulse arrival times for this period exhibit a systematic variation in phase readily explained by light-travel time effects produced by reflex orbital motion about an unseen companion. Our best-fit model to the observations indicates a highly eccen tric orbit, a period of 109 ± 13 days and a minimum mass of 0.5 Mʘ for the companion. Radial velocity variations predicted by this model are not observed, however, nor are these phase variations seen in another independent pulsation, so the origin of the phase variation remains a mystery. Any model involving intrinsic pulsation mechanisms must explain the large (~200 s) phase change with no corresponding change in pulsation amplitude, and it shape, which mimics quite exactly the effects of binary orbital motion.application/pdfengThe astrophysical journal. Chicago. Vol. 357, no. 2, pt. 1 (July 1990), p. 630-637AstrofísicaAnãs brancasEstrelas binariasPulsacoes estelaresStars: binariesStars: individual (G29-38)Stars: pulsationStars: white dwarfsWhole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second periodEstrangeiroinfo:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersioninfo:eu-repo/semantics/openAccessreponame:Repositório Institucional da UFRGSinstname:Universidade Federal do Rio Grande do Sul (UFRGS)instacron:UFRGSORIGINAL000015354.pdf000015354.pdfTexto completo (inglês)application/pdf163414http://www.lume.ufrgs.br/bitstream/10183/108715/1/000015354.pdfc5a64761bff4fbf6ccf74c33cdeb4d11MD51TEXT000015354.pdf.txt000015354.pdf.txtExtracted Texttext/plain176http://www.lume.ufrgs.br/bitstream/10183/108715/2/000015354.pdf.txt6c10bda7ba1c4f86ce155f798a3ccf57MD52THUMBNAIL000015354.pdf.jpg000015354.pdf.jpgGenerated Thumbnailimage/jpeg2089http://www.lume.ufrgs.br/bitstream/10183/108715/3/000015354.pdf.jpg17722250a884041f40b9071444eeb71bMD5310183/1087152022-02-22 05:10:12.773869oai:www.lume.ufrgs.br:10183/108715Repositório de PublicaçõesPUBhttps://lume.ufrgs.br/oai/requestopendoar:2022-02-22T08:10:12Repositório Institucional da UFRGS - Universidade Federal do Rio Grande do Sul (UFRGS)false |
dc.title.pt_BR.fl_str_mv |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
title |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
spellingShingle |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period Winget, Donald Earl Astrofísica Anãs brancas Estrelas binarias Pulsacoes estelares Stars: binaries Stars: individual (G29-38) Stars: pulsation Stars: white dwarfs |
title_short |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
title_full |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
title_fullStr |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
title_full_unstemmed |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
title_sort |
Whole Earth Telescope observations of the white dwarf G29-38 : phase variations of the 615 second period |
author |
Winget, Donald Earl |
author_facet |
Winget, Donald Earl Nather, R. Edward Clemens, J. Christopher Provencal, Judith L. Kleinman, Scot James Bradley, Paul A. Wood, Matthew A. Claver, C.F. Robinson, E.L. Grauer, Albert D. Hine, B.P. Fontaine, Gilles Achilleos, Nicholas Marar, T.M. Krishnan Seetha, S. Ashoka, B.N. O'Donoghue, Darragh Warner, B. Kurtz, Donald W. Martinez, Peter Vauclair, Gérard Chevreton, Michel Augusteijn, T. Paradijs, J. van Hansen, Carl J. Liebert, James Kanaan Neto, Antonio Nemer Kepler, Souza Oliveira |
author_role |
author |
author2 |
Nather, R. Edward Clemens, J. Christopher Provencal, Judith L. Kleinman, Scot James Bradley, Paul A. Wood, Matthew A. Claver, C.F. Robinson, E.L. Grauer, Albert D. Hine, B.P. Fontaine, Gilles Achilleos, Nicholas Marar, T.M. Krishnan Seetha, S. Ashoka, B.N. O'Donoghue, Darragh Warner, B. Kurtz, Donald W. Martinez, Peter Vauclair, Gérard Chevreton, Michel Augusteijn, T. Paradijs, J. van Hansen, Carl J. Liebert, James Kanaan Neto, Antonio Nemer Kepler, Souza Oliveira |
author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author |
dc.contributor.author.fl_str_mv |
Winget, Donald Earl Nather, R. Edward Clemens, J. Christopher Provencal, Judith L. Kleinman, Scot James Bradley, Paul A. Wood, Matthew A. Claver, C.F. Robinson, E.L. Grauer, Albert D. Hine, B.P. Fontaine, Gilles Achilleos, Nicholas Marar, T.M. Krishnan Seetha, S. Ashoka, B.N. O'Donoghue, Darragh Warner, B. Kurtz, Donald W. Martinez, Peter Vauclair, Gérard Chevreton, Michel Augusteijn, T. Paradijs, J. van Hansen, Carl J. Liebert, James Kanaan Neto, Antonio Nemer Kepler, Souza Oliveira |
dc.subject.por.fl_str_mv |
Astrofísica Anãs brancas Estrelas binarias Pulsacoes estelares |
topic |
Astrofísica Anãs brancas Estrelas binarias Pulsacoes estelares Stars: binaries Stars: individual (G29-38) Stars: pulsation Stars: white dwarfs |
dc.subject.eng.fl_str_mv |
Stars: binaries Stars: individual (G29-38) Stars: pulsation Stars: white dwarfs |
description |
Using an extensive set of high-speed photometric observations obtained with the Whole Earth Telescope network, we show that the complex light curve of the ZZ Ceti (DAV) star G29-38 is dominated by a single, constant amplitude period of 615 s during the time span of our observations. The pulse arrival times for this period exhibit a systematic variation in phase readily explained by light-travel time effects produced by reflex orbital motion about an unseen companion. Our best-fit model to the observations indicates a highly eccen tric orbit, a period of 109 ± 13 days and a minimum mass of 0.5 Mʘ for the companion. Radial velocity variations predicted by this model are not observed, however, nor are these phase variations seen in another independent pulsation, so the origin of the phase variation remains a mystery. Any model involving intrinsic pulsation mechanisms must explain the large (~200 s) phase change with no corresponding change in pulsation amplitude, and it shape, which mimics quite exactly the effects of binary orbital motion. |
publishDate |
1990 |
dc.date.issued.fl_str_mv |
1990 |
dc.date.accessioned.fl_str_mv |
2014-12-31T02:10:48Z |
dc.type.driver.fl_str_mv |
Estrangeiro info:eu-repo/semantics/article |
dc.type.status.fl_str_mv |
info:eu-repo/semantics/publishedVersion |
format |
article |
status_str |
publishedVersion |
dc.identifier.uri.fl_str_mv |
http://hdl.handle.net/10183/108715 |
dc.identifier.issn.pt_BR.fl_str_mv |
0004-637X |
dc.identifier.nrb.pt_BR.fl_str_mv |
000015354 |
identifier_str_mv |
0004-637X 000015354 |
url |
http://hdl.handle.net/10183/108715 |
dc.language.iso.fl_str_mv |
eng |
language |
eng |
dc.relation.ispartof.pt_BR.fl_str_mv |
The astrophysical journal. Chicago. Vol. 357, no. 2, pt. 1 (July 1990), p. 630-637 |
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openAccess |
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application/pdf |
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